2011A&A...536A..22P


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.09CET21:56:18

2011A&A...536A..22P - Astronomy and Astrophysics, volume 536A, 22-22 (2011/12-1)

Planck early results. XXII. The submillimetre properties of a sample of galactic cold clumps.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ARNAUD M., ASHDOWN M., AUMONT J., BACCIGALUPI C., BAKER M., BALBI A., BANDAY A.J., BARREIRO R.B., BARTLETT J.G., BATTANER E., BENABED K., BENNETT K., BENOIT A., BERNARD J.-P., BERSANELLI M., BHATIA R., BOCK J.J., BONALDI A., BOND J.R., BORRILL J., BOUCHET F.R., BRADSHAW T., BREMER M., BUCHER M., BURIGANA C., BUTLER R.C., CABELLA P., CANTALUPO C.M., CAPPELLINI B., CARDOSO J.-F., CARR R., CASALE M., CATALANO A., CAYON L., CHALLINOR A., CHAMBALLU A., CHARRA J., CHARY R.-R., CHIANG L.-Y., CHIANG C., CHRISTENSEN P.R., CLEMENTS D.L., COLOMBI S., COUCHOT F., COULAIS A., CRILL B.P., CRONE G., CROOK M., CUTTAIA F., DANESE L., D'ARCANGELO O., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE BRUIN J., DE GASPERIS G., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DELOUIS J.-M., DESERT F.-X., DICK J., DICKINSON C., DOLAG K., DOLE H., DONZELLI S., DORE O., DOERL U., DOUSPIS M., DUPAC X., EFSTATHIOU G., ENSSLIN T.A., ERIKSEN H.K., FINELLI F., FOLEY S., FORNI O., FOSALBA P., FRAILIS M., FRANCESCHI E., FRESCHI M., GAIER T.C., GALEOTTA S., GALLEGOS J., GANDOLFO B., GANGA K., GIARD M., GIARDINO G., GIENGER G., GIRAUD-HERAUD Y., GONZALEZ J., GONZALEZ-NUEVO J., GORSKI K.M., GRATTON S., GREGORIO A., GRUPPUSO A., GUYOT G., HAISSINSKI J., HANSEN F.K., HARRISON D., HELOU G., HENROT-VERSILLE S., HERNANDEZ-MONTEAGUDO C., HERRANZ D., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HORNSTRUP A., HOVEST W., HOYLAND R.J., HUFFENBERGER K.M., JAFFE A.H., JAGEMANN T., JONES W.C., JUILLET J.J., JUVELA M., KANGASLAHTI P., KEIHAENEN E., KESKITALO R., KISNER T.S., KNEISSL R., KNOX L., KRASSENBURG M., KURKI-SUONIO H., LAGACHE G., LAEHTEENMAEKI A., LAMARRE J.-M., LANGE A.E., LASENBY A., LAUREIJS R.J., LAWRENCE C.R., LEACH S., LEAHY J.P., LEONARDI R., LEROY C., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LOWE S., LUBIN P.M., MACIAS-PEREZ J.F., MACIASZEK T., MacTAVISH C.J., MAFFEI B., MAINO D., MANDOLESI N., MANN R., MARIS M., MARTINEZ-GONZALEZ E., MASI S., MASSARDI M., MATARRESE S., MATTHAI F., MAZZOTTA P., McDONALD A., McGEHEE P., MEINHOLD P.R., MELCHIORRI A., MELIN J.-B., MENDES L., MENNELLA A., MEVI C., MINISCALCO R., MITRA S., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORISSET N., MORTLOCK D., MUNSHI D., MURPHY A., NASELSKY P., NATOLI P., NETTERFIELD C.B., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., O'DWYER I.J., ORTIZ I., OSBORNE S., OSUNA P., OXBORROW C.A., PAGANI L., PAJOT F., PALADINI R., PARTRIDGE B., PASIAN F., PASSVOGEL T., PATANCHON G., PEARSON D., PEARSON T.J., PERDEREAU O., PEROTTO L., PERROTTA F., PIACENTINI F., PIAT M., PIERPAOLI E., PLASZCZYNSKI S., PLATANIA P., POINTECOUTEAU E., POLENTA G., PONTHIEU N., POPA L., POUTANEN T., PREZEAU G., PRUNET S., PUGET J.-L., RACHEN J.P., REACH W.T., REBOLO R., REINECKE M., REIX J.-M., RENAULT C., RICCIARDI S., RILLER T., RISTORCELLI I., ROCHA G., ROSSET C., ROWAN-ROBINSON M., RUBINO-MARTIN J.A., RUSHOLME B., SALERNO E., SANDRI M., SANTOS D., SAVINI G., SCHAEFER B.M., SCOTT D., SEIFFERT M.D., SHELLARD P., SIMONETTO A., SMOOT G.F., SOZZI C., STARCK J.-L., STERNBERG J., STIVOLI F., STOLYAROV V., STOMPOR R., STRINGHETTI L., SUDIWALA R., SUNYAEV R., SYGNET J.-F., TAPIADOR D., TAUBER J.A., TAVAGNACCO D., TAYLOR D., TERENZI L., TEXIER D., TOFFOLATTI L., TOMASI M., TORRE J.-P., TRISTRAM M., TUOVINEN J., TUERLER M., TUTTLEBEE M., UMANA G., VALENZIANO L., VALIVIITA J., VARIS J., VIBERT L., VIELVA P., VILLA F., VITTORIO N., WADE L.A., WANDELT B.D., WATSON C., WHITE S.D.M., WHITE M., WILKINSON A., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

We perform a detailed investigation of sources from the Cold Cores Catalogue of Planck Objects (C3PO). Our goal is to probe the reliability of the detections, validate the separation between warm and cold dust emission components, provide the first glimpse at the nature, internal morphology and physical characterictics of the Planck-detected sources. We focus on a sub-sample of ten sources from the C3PO list, selected to sample different environments, from high latitude cirrus to nearby (150pc) and remote (2kpc) molecular complexes. We present Planck surface brightness maps and derive the dust temperature, emissivity spectral index, and column densities of the fields. With the help of higher resolution Herschel and AKARI continuum observations and molecular line data, we investigate the morphology of the sources and the properties of the substructures at scales below the Planck beam size. The cold clumps detected by Planck are found to be located on large-scale filamentary (or cometary) structures that extend up to 20pc in the remote sources. The thickness of these filaments ranges between 0.3 and 3pc, for column densities NH2∼0.1 to 1.6x1022cm–2, and with linear mass density covering a broad range, between 15 and 400M/pc. The dust temperatures are low (between 10 and 15K) and the Planck cold clumps correspond to local minima of the line-of-sight averaged dust temperature in these fields. These low temperatures are confirmed when AKARI and Herschel data are added to the spectral energy distributions. Herschel data reveal a wealth of substructure within the Planck cold clumps. In all cases (except two sources harbouring young stellar objects), the substructures are found to be colder, with temperatures as low as 7K. Molecular line observations provide gas column densities which are consistent with those inferred from the dust. The linewidths are all supra-thermal, providing large virial linear mass densities in the range 10 to 300M/pc, comparable within factors of a few, to the gas linear mass densities. The analysis of this small set of cold clumps already probes a broad variety of structures in the C3PO sample, probably associated with different evolutionary stages, from cold and starless clumps, to young protostellar objects still embedded in their cold surrounding cloud. Because of the all-sky coverage and its sensitivity, Planck is able to detect and locate the coldest spots in massive elongated structures that may be the long-searched for progenitors of stellar clusters.

Abstract Copyright:

Journal keyword(s): ISM: clouds - dust, extinction - stars: formation - ISM: structure - submillimeter: ISM - stars: protostars

CDS comments: Table 1 Sources G20.7+20.0, G109.8+2.7 and G107.2+5.5 not identified (incomplete format). PCC288-P1 and PCC288-P2 not in SIMBAD.

Simbad objects: 34

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Number of rows : 34

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME NCP reg 00 00 00 +90 00.0           ~ 135 0
2 PLCKECC G131.72+09.70 cor 02 39 57.6 +70 42 12           ~ 6 0
3 LDN 1355 DNe 02 52.7 +69 02           ~ 15 0
4 LDN 1358 DNe 02 55 54 +69 20.8           ~ 9 0
5 NAME Per Arm PoG 03 30 +45.0           ~ 1202 0
6 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 223 0
7 Ass Per OB 2 As* 03 42.2 +33 26           ~ 302 0
8 PLCKECC G161.34-09.32 cor 04 15 21.6 +37 53 39           ~ 5 0
9 NAME Auriga reg 04 20 00.0 +38 05 00           ~ 164 0
10 PLCKECC G126.62+24.54 cor 04 23 17.0 +85 47 12           ~ 4 0
11 NAME MCLD 126.6+24.5 MoC 04 23 55.8 +85 46 47           ~ 27 0
12 LBN 126.54+24.68 HII 04 26 +85.9           ~ 1 0
13 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3335 0
14 PLCKECC G176.17-02.10 cor 05 27 55.2 +31 01 35           ~ 5 0
15 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 466 0
16 M 42 HII 05 35 17.3 -05 23 28           ~ 3664 0
17 NAME Ori Complex Cld 05 35.3 -05 23           ~ 319 0
18 TGU H1490 DNe 05 40.7 -09 03           ~ 4 0
19 TGU H1490 P43 DNe 05 52.7 -09 28           ~ 2 0
20 PLCKECC G215.41-16.39 cor 05 56 58.0 -09 32 28           ~ 7 0
21 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1090 2
22 NAME Vela-D Molecular Cloud MoC 08 39 -41.0           ~ 42 0
23 NAME VELA MOL RIDGE MoC 08 53 -45.0           ~ 130 0
24 DCld 276.9+01.7 DNe 09 50 45 -51 44.4           ~ 4 0
25 NAME Musca Filament PoC 10 54 -74.0           ~ 20 0
26 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 160 1
27 NAME Musca Cld 12 23 -71.3           ~ 152 0
28 PLCKECC G300.87-08.95 cor 12 25 26.0 -71 43 09           ~ 3 0
29 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2944 0
30 NAME Cometary Nebula ~ 20 20.2 +37 10           ~ 6 0
31 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 630 2
32 IRAS 22176+6303 SFR 22 19 17.978 +63 18 52.92           ~ 588 0
33 NAME Ass Cep OB 3b As* 22 55 00.0 +62 35 00           ~ 32 0
34 NAME Cep Flare MoC 23 34 +72.0           ~ 98 0

    Equat.    Gal    SGal    Ecl

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2019.12.09-21:56:18

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